Radiation pressure in galactic disks: stability, turbulence, and winds in the single-scattering limit

TL;DR

This study investigates the stability and turbulence driven by radiation pressure in galactic disks within the single-scattering limit, revealing that radiation induces turbulence but does not significantly support star-forming disks against gravity.

Contribution

It provides a detailed stability analysis and multidimensional radiation-hydrodynamic simulations of dusty gas columns in the single-scattering regime, a regime less explored in prior work.

Findings

Radiation induces convective-like turbulence with Mach numbers up to 2.

Turbulent energy densities are about 1-10% of the radiation energy density.

Radiation pressure alone does not significantly support star-forming disks against gravity.

Abstract

The radiation force on dust grains may be dynamically important in driving turbulence and outflows in rapidly star-forming galaxies. Recent studies focus on the highly optically-thick limit relevant to the densest ultra-luminous galaxies and super star clusters, where reprocessed infrared photons provide the dominant source of electromagnetic momentum. However, even among starburst galaxies, the great majority instead lie in the so-called "single-scattering" limit, where the system is optically-thick to the incident starlight, but optically-thin to the re-radiated infrared. In this paper we present a stability analysis and multidimensional radiation-hydrodynamic simulations exploring the stability and dynamics of isothermal dusty gas columns in this regime. We describe our algorithm for full angle-dependent radiation transport based on the discontinuous Galerkin finite element method. For a range of near-Eddington fluxes, we show that the medium is unstable, producing convective-like motions in a turbulent atmosphere with a scale height significantly inflated compared to the gas pressure scale height and mass-weighted turbulent energy densities of $\sim 0.01-0.1$ of the midplane radiation energy density, corresponding to mass-weighted velocity dispersions of Mach number $\sim 0.5-2$. Extrapolation of our results to optical depths of $10^3$ implies maximum turbulent Mach numbers of $\sim20$. Comparing our results to galaxy-averaged observations, and subject to the approximations of our calculations, we find that radiation pressure does not contribute significantly to the effective supersonic pressure support in star-forming disks, which in general are substantially sub-Eddington. We further examine the time-averaged vertical density profiles in dynamical equilibrium and comment on implications for radiation-pressure-driven galactic winds.